Iron isotopes in chondrules: Implications for the role of evaporation during chondrule formation

Details Iron isotopes in chondrules: Implications for the role of evaporation during chondrule formation Iron isotopes in chondrules: Implications for the role of evaporation during chondrule formation

Mar 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001m%26ps...36..419a&link_type=abstract

Meteoritics & Planetary Science, vol. 36, no. 3, p. 419-428

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Scientific paper

We have measured the ?57Fe of olivines in nine Chainpur chondrules. All are within error of normal (typically 2?=1-2
=1). Most of the chondules could not have lost more than ~20% of their FeO by Rayleigh evaporation and none can have lost more than ~61%. Yet, the range of Fo contents in these chondrules is Fo78-Fo99.9. The isotopic compositions of the chondrules clearly demonstrate that, for instance, Type I chondrules cannot form from Type II chondrules by evaporation of FeO under Rayleigh conditions. The isotopic compositions also place constraints on the minimum cooling rates these chondrules could have experienced. These cooling rates must also be equal to or slower than those required to produce the chondrule textures. Assuming flash heating and evaporation rates like those measured in vacuum, the minimum cooling rates necessary to prevent detectable Fe isotopic fractionation via Rayleigh evaporation approach those needed to produce barred and porphyritic textures. The presence of hydrogen in the Nebula, non-linear cooling and other effects will all tend to increase the cooling rates required to prevent ?57Fe>1-2
=1, perhaps by as much as 1-2 orders of magnitude. The two most likely ways that the cooling rates required to prevent ?57Fe>1-2
=1 can be kept below those needed to produce barred and porphyritic textures are: (1) the pH2 in the Nebula was low enough to keep evaporation rates close to those in vacuum, or (2) back reaction of chondrules with Fe in the gas suppressed isotopic fractionation.

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